ABHT(QMC-RMF3)
Abstract
An out-of-equilibrium and finite-temperature equation of state (EoS). The core is homogeneous n, p, e matter computed using a relativistic mean-field theory constrained by chiral effective field theory calculations of pure neutron matter at zero temperature (from 0.08 fm−3 to 0.32 fm−3), by properties of isospin-symmetric nuclear matter around nuclear saturation density, and by astrophysical observations of neutron stars [ABHT_2022 ]. To describe nuclear matter over the physically-relevant range of densities for use in, e.g., simulations of neutron star mergers, we attach the HS(IUF) EoS [ HSNP_2010 ][FHPSP_2010 ] in a thermodynamically consistent manner to model inhomogeneous nuclear matter at low densities. See Ref. [ABHT_2023 ] for more details about this EoS.
| Nparam | = | 3 |
| Particles | = | None |
| T min | = | 1.00e-01 |
| T max | = | 1.58e+02 |
| T pts | = | 81 |
| nb min | = | 1.00e-12 |
| nb max | = | 1.58e+00 |
| nb pts | = | 306 |
| Y min | = | 1.00e-02 |
| Y max | = | 6.00e-01 |
| Y pts | = | 60 |
Nuclear Matter Properties
| ns | = | 0.1546 | fm-3 |
| E0 | = | -16.39 | Mev |
| K | = | 231.3 | Mev |
| K' | = | -290.3 | Mev |
| J | = | 31.29 | Mev |
| L | = | 47.2 | Mev |
| Ksym | = | 28.5 | MeV |
Neutron Star Properties
| Mmax | = | 1.95 | Msun |
| MDU,e | = | N/A | Msun |
| RMmax | = | 10.16 | km |
| R1.4 | = | 11.81 | km |
References
References to the original work:
- [HSNP_2010] M. Hempel and J. Schaffner-Bielich, Nucl. Phys. A 837, 210 (2010)
- [FHPSP_2010] F.J. Fattoyev, C.J. Horowitz, J. Piekarewicz, and G. Shen, Phys. Rev. C 82, 055803 (2010)
- [ABHT_2022] M. G. Alford, L. Brodie, A. Haber, and I. Tews, Phys. Rev. C 106, 055804 (2022)
- [ABHT_2023] M. G. Alford, L. Brodie, A. Haber, and I. Tews, Phys.Scripta 98, 125302 (2023)
Data sheet
Data
| eos.zip (167.83 MB) |
| eos.zip_checksum.txt |
Single files |
| eos.mr |
| eos.compo |
| eos.init |
| eos.micro |
| eos.thermo |
| eos.t |
| eos.nb |
| eos.yq |
| eos.thermo.ns |
| eos.nb.ns |